Flared Disc Project：RXTE和ASCA对X 1822-371的观察

我们报告了关于流行的RXTE和同步ASCA数据，针对这一 eclipsing低质量X射线二元体X 1822-371进行分析。我们的光谱分析显示，各种简单模型都能较好地拟合光谱。在这些模型中，我们通过相位分辨拟合详细探索了两种模型。这两种模型分别代表极其致密的和极其稀薄的天体冠。尽管在高能范围仍存在系统残差，但整体光谱形状仍被良好近似。将这两个基本模型拟合到X射线光度曲线，该曲线显示出正弦性变化，被解释为来自高度不透明盘边缘的吸收，其高度变化。我们推断的几何结构与前述研究一致：盘边缘延伸至潮汐截断半径，而天体冠的半径（近似为球形）非常接近圆化半径。RXTE数据的时序分析显示，从硬X射线到软X射线之间存在时滞，与从拟合中推断的冠层大小一致。Neither spectra nor light curve fits allow us to rule out either model, leaving a key ingredient of the X 1822-371 puzzle unsolved. Furthermore, while previous studies were consistent with the central object being a 1.4 Msol neutron star, which has been adopted as the best guess scenario for this system, our light curve fits show that a white dwarf or black hole primary can work just as well. Based on previously published estimates of the orbital evolution of X 1822-371, however, we suggest that this system contains either a neutron star or a low mass (~ 2.5 Msol) black hole and is in a transitional state of duration shortward of 10^7 years.